A multiwavelength timing analysis of the eclipsing polar DP Leo

Abstract

We present an analysis of the X-ray light curves of the magnetic cataclysmic variable DP Leo using recently per- formed XMM Newton EPIC and archival published and unpublished ROSAT PSPC observations. We combine the timings of the X-ray eclipses with timings derived from archival HST-observations and new optical observations with the photon counting OPTIMA camera. We determine the eclipse length at X-ray wavelengths to be 235 5 s, slightly longer than at ultra-violet wavelengths, where it lasts 225 s. A new orbital ephemeris is derived which connects the more than 120 000 binary cycles covered since 1979. It has a highly significant quadratic term, implying an orbital period change of ˙ P = 4:4 10 12 ss 1 , two orders of magnitude larger than being compatible with braking by gravitational radiation only. Over the last twenty years, the optical and X-ray bright phases display a continuous shift with respect to the eclipse center by2:1 yr 1 .O ver the last 8.5 years the shift of the X-ray bright phase is2:5 yr 1 . We interpret this as evidence of an asynchronously rotating white dwarf although synchronization oscillations cannot be ruled out completely. If the observed phase shift continues, a funda- mental rearrangement of the accretion geometry must occur on a time-scale of some ten years. Applying model atmosphere spectra to optical/UV eclipse light curves, we determine the temperature and mass of the white dwarf, the temperature and size of the optical/UV emitting spot and the distance to DP Leo to be Twd = 13 500 K, Mwd ' 0:6 M, Tspot = 32 000 K, Aspot ' 0:1 Awd ,a ndD= 400 pc, respectively. The implied inclination and mass ratio are i= 79:5 and Q= Mwd=M2 = 6:7. DP Leo is marginally detected at eclipse phase in X-rays. The upper limit eclipse flux is consistent with an origin on the late-type secondary, LX' 2:5 10 29 ergs s 1 (0.20 7.55 keV), at a distance of 400 pc.